The Effect of f(R, T) Modified Gravity on the Mass and Radius of Pulsar HerX1

Abstract

Millisecond pulsars are the perfect testable to examine potential matter-geometry coupling and its physical consequences in the context of the recent Neutron Star Interior Composition Explorer discoveries. We apply the field equations of modified gravity, f(R, T) = R + α T, to a spherically symmetric spacetime, where R is the Ricci scalar, α is a dimensional parameter, and T is the matter of the geometry. Five unknown functions are present in the output system of differential equations, which consists of three equations. To close the system, we make explicit assumptions about the anisotropy and the radial metric potential, g rr . We then solve the output differential equations and derive the explicit forms of the components of the energy-momentum tensor, i.e., density, radial, and tangential pressures. We look into the possibility that all of the physical parameters in the star can be reexpressed in terms of α and the compactness parameters, C = 2 GM Rc−2. We show that, for a given mass, the size permitted by Einstein’s general relativity is less due to the matter-geometry coupling in f(R, T). The validity of the hypothesis was validated by observations from an extra 21 pulsars. To achieve a surface density that is compatible with a neutron core at nuclear saturation density, the mass–radius curve enables masses up to 3.35M ⊙. We emphasize that although there is no assumption of an equation of state, the model fits well with a linear behavior. When comparing the surface densities of these 20 pulsars, we divided them into three groups. We show that these three groups are compatible with neutron cores.

Constraining quadratic f(R) gravity from astrophysical observations of the pulsar J0704+6620

“…In spite of the capability of the model to lower the speed of sound in comparison to the GR or quadratic gravity with positive ϵ cases, it is still above the conjectured conformal upper bound on the maximum sound speed c 2 s = c 2 /3. This result may favor matter-geometry nonminimal coupling scenario to provide better framework for treating that issue as suggested by [26,37,84].…”

Extending Finch-Skea isotropic model to anisotropic domain in modified f(, T ) gravity

“…Multiple minimal/non-minimal models have been proposed in this scenario, among them   x + 2 gained great attention in the literature due to its linear nature. Nashed [11] discussed various pulsars in this linear gravity model and solved the differential equations by making an explicit assumption regarding the anisotropy and radial component of the metric. They found that the estimated masses of these pulsars are in accordance with the observed ones.…”

Moment of inertia and compactness of quark stars within the context of f(R, T, L m ) gravity

“…On the other hand, Harko and collaborators [57] proposed another extension of standard GR, the f (R, T) modified gravity theories, where the gravitational Lagrangian is given by an arbitrary function of the Ricci scalar R and of the trace of the energy-momentum tensor T. The cosmological consequences [58][59][60][61][62][63][64][65][66][67][68][69] and applications to compact stars [70][71][72][73][74][75][76][77][78][79][80][81][82][83] of such a theory have been addressed by several authors in recent years. See further [84][85][86][87] for a novel scalar-tensor representation of f (R, T) gravity.…”